Internal gravity waves in magnetic stars

内部重力波（或g模）在恒星的辐射区中传播，例如在太阳的辐射核心。这些波可以在恒星中被邻近对流区的湍流、流体不稳定性或伴星（如近轨道热木星）的引力潮汐强迫所激发。像太阳这样的恒星是有磁性的物体。例如，太阳辐射带被认为是一个大规模磁场的港湾，这被认为是解释核心的近似固体旋转。然而，磁场对重力波传播的影响，以及对重力波稳定性和耗散的影响还没有得到充分的研究。这一理论和计算项目将侧重于研究磁场对恒星和行星内部重力波的影响。目标是了解磁场对这些波的影响，并确定在系外行星或近距离双星系统以及红巨星核心中潮汐激发的重力波的任何天体物理学意义。

Internal gravity waves (or g-modes) propagate in the radiation zones of stars, such as in the radiative core of the Sun. These waves can be excited in stars by turbulence in neighbouring convection zones, by fluid instabilities, or by gravitational tidal forcing due to a companion, such as a closely orbiting hot Jupiter. Stars such as the Sun are magnetised objects. For example, the solar radiation zone is believed to harbour a large-scale magnetic field, which is thought to explain the approximate solid body rotation of the core. However, the effects of magnetic fields on the propagation of gravity waves, and on their stability and dissipation has not been fully explored. This theoretical and computational project will focus on studying aspects of the effects of magnetic fields on gravity waves in stellar and planetary interiors. The goal is to understand the effects of magnetic fields on these waves, and to determine any astrophysical implications for gravity waves that are tidally-excited in exoplanet or close binary systems, as well as the in cores of red giant stars.